Hypernova signatures in the late rebrightening of GRB 050525A

M. Della Valle; D. Malesani; J. S. Bloom; S. Benetti; G. Chincarini; P. D'Avanzo; R. J. Foley; S. Covino; A. Melandri; S. Piranomonte; G. Tagliaferri; L. Stella; R. Gilmozzi; L. A. Antonelli; S. Campana; H. W. Chen; P. Filliatre; F. Fiore; D. Fugazza; N. Gehrels; K. Hurley; I. F. Mirabel; L. J. Pellizza; L. Piro; J. X. Prochaska

doi:10.1086/504636

Hypernova signatures in the late rebrightening of GRB 050525A

M. Della Valle, D. Malesani, J. S. Bloom, S. Benetti, G. Chincarini, P. D'Avanzo, R. J. Foley, S. Covino, A. Melandri, S. Piranomonte, G. Tagliaferri, L. Stella, R. Gilmozzi, L. A. Antonelli, S. Campana, H. W. Chen, P. Filliatre, F. Fiore, D. Fugazza, N. GehrelsK. Hurley, I. F. Mirabel, L. J. Pellizza, L. Piro, J. X. Prochaska

Astronomy

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Abstract

We report observations of GRB 050525A, for which a Gemini North spectrum shows its redshift to be z = 0.606. This is the third closest long GRB discovered by Swift. We observed its afterglow using the VLT, Gemini, and TNG telescopes to search for an associated supernova. We find that the early-time light curve is described by a broken power law with a break at t ∼ 0.3 days after the burst. About 5 days after the burst, a flattening is apparent, followed by a further dimming. Both the magnitude and the shape of the light curve suggest that a supernova was emerging during the late decay of the afterglow. This supernova, named SN 2005nc, had a rise time faster than SN 1998bw and a long-lasting maximum. A spectrum obtained about 20 days (rest frame) after the GRB resembles the spectrum of SN 1998bw obtained close to maximum light.

Original language	English (US)
Pages (from-to)	L103-L106
Journal	Astrophysical Journal
Volume	642
Issue number	2 II
DOIs	https://doi.org/10.1086/504636
State	Published - May 10 2006

Keywords

Gamma rays: bursts
Supernovae: individual (GRB 050525A)

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Online availability

10.1086/504636

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Della Valle, M., Malesani, D., Bloom, J. S., Benetti, S., Chincarini, G., D'Avanzo, P., Foley, R. J., Covino, S., Melandri, A., Piranomonte, S., Tagliaferri, G., Stella, L., Gilmozzi, R., Antonelli, L. A., Campana, S., Chen, H. W., Filliatre, P., Fiore, F., Fugazza, D., ... Prochaska, J. X. (2006). Hypernova signatures in the late rebrightening of GRB 050525A. Astrophysical Journal, 642(2 II), L103-L106. https://doi.org/10.1086/504636

Della Valle, M, Malesani, D, Bloom, JS, Benetti, S, Chincarini, G, D'Avanzo, P, Foley, RJ, Covino, S, Melandri, A, Piranomonte, S, Tagliaferri, G, Stella, L, Gilmozzi, R, Antonelli, LA, Campana, S, Chen, HW, Filliatre, P, Fiore, F, Fugazza, D, Gehrels, N, Hurley, K, Mirabel, IF, Pellizza, LJ, Piro, L & Prochaska, JX 2006, 'Hypernova signatures in the late rebrightening of GRB 050525A', Astrophysical Journal, vol. 642, no. 2 II, pp. L103-L106. https://doi.org/10.1086/504636

@article{8b084ceafa6f48bb9ba49332765abf79,

title = "Hypernova signatures in the late rebrightening of GRB 050525A",

abstract = "We report observations of GRB 050525A, for which a Gemini North spectrum shows its redshift to be z = 0.606. This is the third closest long GRB discovered by Swift. We observed its afterglow using the VLT, Gemini, and TNG telescopes to search for an associated supernova. We find that the early-time light curve is described by a broken power law with a break at t ∼ 0.3 days after the burst. About 5 days after the burst, a flattening is apparent, followed by a further dimming. Both the magnitude and the shape of the light curve suggest that a supernova was emerging during the late decay of the afterglow. This supernova, named SN 2005nc, had a rise time faster than SN 1998bw and a long-lasting maximum. A spectrum obtained about 20 days (rest frame) after the GRB resembles the spectrum of SN 1998bw obtained close to maximum light.",

keywords = "Gamma rays: bursts, Supernovae: individual (GRB 050525A)",

author = "{Della Valle}, M. and D. Malesani and Bloom, {J. S.} and S. Benetti and G. Chincarini and P. D'Avanzo and Foley, {R. J.} and S. Covino and A. Melandri and S. Piranomonte and G. Tagliaferri and L. Stella and R. Gilmozzi and Antonelli, {L. A.} and S. Campana and Chen, {H. W.} and P. Filliatre and F. Fiore and D. Fugazza and N. Gehrels and K. Hurley and Mirabel, {I. F.} and Pellizza, {L. J.} and L. Piro and Prochaska, {J. X.}",

note = "Funding Information: M. D. V. thanks the Kavli Institute for Theoretical Physics at the University of California at Santa Barbara, where this work was completed, for its hospitality. This research was supported in part by the National Science Foundation under grant PHY99-0974. J. S. B., J. X. P., and H.-W. C. are partially supported by NASA/Swift grant NNG05GF55G. K. H. is grateful for support under NASA grant FDNAG5-9210. This work is based on observations obtained at ESO, TNG, and Gemini Observatories. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.",

year = "2006",

month = may,

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doi = "10.1086/504636",

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TY - JOUR

T1 - Hypernova signatures in the late rebrightening of GRB 050525A

AU - Della Valle, M.

AU - Malesani, D.

AU - Bloom, J. S.

AU - Benetti, S.

AU - Chincarini, G.

AU - D'Avanzo, P.

AU - Foley, R. J.

AU - Covino, S.

AU - Melandri, A.

AU - Piranomonte, S.

AU - Tagliaferri, G.

AU - Stella, L.

AU - Gilmozzi, R.

AU - Antonelli, L. A.

AU - Campana, S.

AU - Chen, H. W.

AU - Filliatre, P.

AU - Fiore, F.

AU - Fugazza, D.

AU - Gehrels, N.

AU - Hurley, K.

AU - Mirabel, I. F.

AU - Pellizza, L. J.

AU - Piro, L.

AU - Prochaska, J. X.

N1 - Funding Information: M. D. V. thanks the Kavli Institute for Theoretical Physics at the University of California at Santa Barbara, where this work was completed, for its hospitality. This research was supported in part by the National Science Foundation under grant PHY99-0974. J. S. B., J. X. P., and H.-W. C. are partially supported by NASA/Swift grant NNG05GF55G. K. H. is grateful for support under NASA grant FDNAG5-9210. This work is based on observations obtained at ESO, TNG, and Gemini Observatories. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests.

PY - 2006/5/10

Y1 - 2006/5/10

N2 - We report observations of GRB 050525A, for which a Gemini North spectrum shows its redshift to be z = 0.606. This is the third closest long GRB discovered by Swift. We observed its afterglow using the VLT, Gemini, and TNG telescopes to search for an associated supernova. We find that the early-time light curve is described by a broken power law with a break at t ∼ 0.3 days after the burst. About 5 days after the burst, a flattening is apparent, followed by a further dimming. Both the magnitude and the shape of the light curve suggest that a supernova was emerging during the late decay of the afterglow. This supernova, named SN 2005nc, had a rise time faster than SN 1998bw and a long-lasting maximum. A spectrum obtained about 20 days (rest frame) after the GRB resembles the spectrum of SN 1998bw obtained close to maximum light.

AB - We report observations of GRB 050525A, for which a Gemini North spectrum shows its redshift to be z = 0.606. This is the third closest long GRB discovered by Swift. We observed its afterglow using the VLT, Gemini, and TNG telescopes to search for an associated supernova. We find that the early-time light curve is described by a broken power law with a break at t ∼ 0.3 days after the burst. About 5 days after the burst, a flattening is apparent, followed by a further dimming. Both the magnitude and the shape of the light curve suggest that a supernova was emerging during the late decay of the afterglow. This supernova, named SN 2005nc, had a rise time faster than SN 1998bw and a long-lasting maximum. A spectrum obtained about 20 days (rest frame) after the GRB resembles the spectrum of SN 1998bw obtained close to maximum light.

KW - Gamma rays: bursts

KW - Supernovae: individual (GRB 050525A)

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U2 - 10.1086/504636

DO - 10.1086/504636

M3 - Article

AN - SCOPUS:33746087278

SN - 0004-637X

VL - 642

SP - L103-L106

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 II

ER -

Hypernova signatures in the late rebrightening of GRB 050525A

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